|Title||Shocked gas in RR Tel|
|Author||Dr Rosario Gonzalez-Riestra|
|Description||RR Tel is an extraordinary laboratory for spectroscopic studies of low density astrophysical plasmas. Its optical and ultraviolet spectrum is extremely rich in emission lines which cover a wide range in excitation and ionization stages. Its X-ray spectrum is dominated by a supersoft component at energies below 0.5 keV, but there is an additional, weaker hard excess. This emission can been attributed to gas ionized by the collision between the winds of the two component of the system, but the data available so far do not allow to draw any conclusion. A good quality X-ray high resolution spectrum of RR Tel will be crucial to understand the physical processes that are taking place in the system, in particular in the collision shock of the winds from the two stars.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2010-05-16T00:00:00Z, 055115, 17.56_20190403_1200. https://doi.org/10.5270/esa-nghbmze|